The Missing Satellite Problem Outside of the Local Group. II. Statistical Properties of Satellites of Milky Way-like Galaxies

TL;DR

This study observes satellite galaxies around seven Milky Way-like galaxies outside the Local Group, finding similarities and differences with the Milky Way satellites, and highlighting the diversity in satellite properties and distributions.

Contribution

First statistical analysis of satellite galaxies around MW-like galaxies outside the Local Group using Subaru data, revealing variations in satellite properties and distributions.

Findings

Satellite luminosity functions are similar to MW satellites but vary among hosts.

More massive hosts tend to have more satellites.

Satellite spatial distribution outside LG shows no concentration or alignment.

Abstract

We present a new observation of satellite galaxies around seven Milky Way (MW)-like galaxies located outside of the Local Group (LG) using Subaru/Hyper Suprime-Cam imaging data to statistically address the missing satellite problem. We select satellite galaxy candidates using magnitude, surface brightness, S\'{e}rsic index, axial ratio, full width half maximum, and surface brightness fluctuation cuts, followed by visual screening of false-positives such as optical ghosts of bright stars. We identify 51 secure dwarf satellite galaxies within the virial radius of nine host galaxies, two of which are drawn from the pilot observation presented in Paper I. We find that the average luminosity function of the satellite galaxies is consistent with that of the MW satellites, although the luminosity function of each host galaxy varies significantly. We observe an indication that more massive hosts tend to have a larger number of satellites. Physical properties of the satellites such as the size-luminosity relation is also consistent with the MW satellites. However, the spatial distribution is different; we find that the satellite galaxies outside of LG shows no sign of concentration or alignment, while that of the MW satellites is more concentrated around the host and exhibits a significant alignment. As we focus on relatively massive satellites with $M_V<-10$, we do not expect that the observational incompleteness can be responsible here. This trend might represent a peculiarity of the MW satellites, and further work is needed to understand its origin.